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The fraction of ionized gas in the Warm Hot Intergalactic Medium inducestemperature anisotropies on the Cosmic Microwave Background similar to those ofclusters of galaxies. The Sunyaev-Zel'dovich anisotropies due to these lowdensity, weakly non-linear, baryon filaments can not be distinguished from thatof clusters using frequency information, but they can be separated since theirangular scales are very different. To determine the relative contribution ofthe WHIM SZ signal to the radiation power spectrum of temperature anisotropies,we explore the parameter space of the concordance LCDM model using Monte CarloMarkov Chains and the Wilkinson Microwave Anisotropy Probe 7yr and South PoleTelescope data. We find marginal evidence of a contribution by diffuse gas,with amplitudes of A_WHIM=10-20 muK^2, but the results are also compatible witha null contribution from the WHIM, allowing to set an upper limit of A_WHIM <43 muK^2 (95.4% C.L.). The signal produced by galaxy clusters remains atA_CL=4.5 muK^2, a value similar to what is obtained when no WHIM is included.From the measured WHIM amplitude we constrain the temperature-density phasediagram of the diffuse gas, and find it to be compatible with numericalsimulations. The corresponding baryon fraction in the WHIM varies from 0.43 to0.47, depending on model parameters. Planck data could set tighter constraintson the temperature-density relation.

Constraints on the Sunyaev-Zel'dovich signal from the Warm Hot Intergalactic Medium from WMAP and SPT data